CCD Imaging in amateur professional astronomy What is

CCD Imaging in amateur & professional astronomy What is a CCD?

Introduction We will examine the following: 1. What is a CCD 2. Advantages of CCDs (particularly over older technologies like photography) 3. How CCDs work

What is a CCD? The acronym CCD stands for Charge Coupled Device. CCDs were invented at Bell Laboratories in the early 1970 s. They were originally designed as computer memory but it quickly became apparent that there were other uses for them. Their primary use today is as a solid-state imaging device. It is this application which has revolutionised astronomy and which we will study further in these Activities.

Astronomical use of CCDs In this discussion of CCDs we will only consider their astronomical use. CCDs are in widespread use today in all manner of devices (video and still cameras, scanners etc. ) but none of these applications are as demanding as astronomy. Most CCDs are used in places where there is plenty of light available and so concerns of efficiency are not relevant. Exposures are brief and so noise sources are unimportant. The subject matter is forgiving and so cosmetic blemishes are noticed. Alas, this is not so when trying to detect a distant galaxy.

Advantages of CCDs over film CCDs have a higher quantum efficiency (QE) than film. QE is a measure of how efficient a device is in turning input energy (in this case light) into a measurable signal. Greater efficiency means that more data can be gathered in a shorter time, or that in the same time you can measure a fainter signal. Professional CCD Best film Amateur CCD

Advantages of CCDs over film CCDs have a linear response to light. i. e. the measured signal is directly proportional to the amount of light which was received. This is not true for film. A linear response means that if the exposure is doubled, then the measurable signal will double. Also, twice the signal means the source is twice as bright. CCD linear response Film non-linear response

More Advantages of CCDs over film • CCDs have a wide dynamic range. Coupled with their linearity they can measure both very faint targets and very bright ones. • CCDs are dimensionally stable. The sensing elements (pixels – or picture elements) are laid out in a regular grid formed on the silicon substrate. This makes them excellent for most forms of positional measurement. • CCDs are digital and so modern computers can be put to use in processing the images. No more messing about with photographic chemicals or working in the dark.

Advantages of CCDs This all adds up to a revolution in astronomy: The increase in QE over film is like making your telescope into a much bigger one - effectively allowing a 1 -m telescope to perform like a 4 -m. The accuracy of CCDs in both linearity and stability means the measurements made are of the highest quality, and a wider band of the spectrum is utilised. The digital nature of CCDs allows new techniques to be devised, both in taking the data and extracting the most from it.

How do CCDs work? There are 4 basic stages to CCD operation. • Light (photons) is converted to a charge (electrons) by the photoelectric effect in a layer of silicon. • The charge is accumulated in “wells” during the exposure. • At the end of the exposure the CCD is “read out” - the charge is shifted to the readout register. • Finally, the charge in each pixel is measured.

How do CCDs work? – charge collection An analogy is useful to picture the mechanisms involved in how CCDs collect, transfer and count charge. Imagine an array of buckets ready to catch rain. A single master rain gauge will be used to measure the amount of rain caught in each bucket. The buckets are connected by siphon pumps. Rain gauge Siphon pump Bucket

How do CCDs work? – charge transfer To measure the rain in each bucket (after the rain has stopped), the siphon pumps are used to move the accumulated rain towards the master rain gauge. Different buckets hold different amounts of rain

How do CCDs work? – charge transfer First, the end line of buckets are emptied into the empty row lined up with the master gauge. Contents of all buckets move to left

How do CCDs work? – charge counting Then each bucket in turn is siphoned into the master gauge for measuring. After each measurement, the master gauge must be emptied before a new measure can be taken. Rain gauge is emptied

How do CCDs work? – charge counting Then each bucket in turn is siphoned into the master gauge for measuring. After each measurement, the master gauge must be emptied before a new measure can be taken. Rain gauge is emptied

How do CCDs work? – charge counting Then each bucket in turn is siphoned into the master gauge for measuring. After each measurement, the master gauge must be emptied before a new measure can be taken. Rain gauge is emptied

How do CCDs work? This shift-and-measure is carried on until all the water along the “readout register” has been measured. The remaining water to be measured is siphoned along into the now empty buckets (the readout register) and the process of shifting-and-measuring is repeated.

How do CCDs work? In the previous analogy, the raindrops represent photons. The accumulated water represents the charge detected by the CCD. The buckets represent pixels on the CCD (and their depth represents the well depth, or how much charge each pixel can hold). The siphon pumps represent the CCD shift registers. The master gauge is the sense capacitor (and the fineness of the graduations represents the measurement accuracy).

How do CCDs work? Of course CCDs are not quite so simple, but the underlying electronics does a good job at mimicking the analogy. CCDs are actually the most complex electronic circuits fabricated today, mainly because of their size and need for perfection over large areas of silicon. This makes them expensive, too! You should have been able to spot from the analogy some of the potential problems associated with CCDs. By examining these areas we will get a better understanding of how they work. Lets start by looking at the individual pixels.

CCD Imaging CCD imaging can turn this raw image. . . NGC 2736, part of the Vela SN remnant. Imaged with 20 cm f/4· 5 Newtonian and Cookbook 245 CCD camera. into this. . .